Using the equation of state of the neutron star matter, we can
calculate the neutron star mass and radius as a function of
central mass density, \(\epsilon _{\rm c}\) , by numerically
integrating the general relativistic equation of hydrostatic
equilibrium, Tolman-Oppenheimer-Volkoff (TOV) equation
[1]},
\(\frac{dP}{dr}=-\frac{G}{r^2}[\epsilon (r) +P(r)/c^2]\frac{m(r)+4\pi r^3P(r)/c^2}{1-\frac{2Gm(r)}{rc^2}},\) 
